Quasar Death Martin Elvis Charles L. Steinhardt1, Heng Hao2, Monica Young3, Guido Risaliti4, Francesca Civano Harvard-Smithsonian Center for Astrophysics and 1. IPMU, Univ. Tokyo; 2. SISSA, 3. Penn State Univ.; 4. INAF, Arcetri, Italy MPIA Heidelberg, July 2011 Why Study Quasars? Astronomy: 100,000 quasars in the ROSAT X-ray sky Astrophysics: Gravity powered Not fusion. Cosmology: Co-evolution of galaxies and supermassive black holes Relativistic jets Physics: Reynolds C. Light bending near the Event horizon MPIA Heidelberg, July 2011 The 7 Ages of Supermassive Black Holes 1. Birth Ignorant 2. Rapid growth – by z=7 No data 3. Merger growth Know a little 4. Quasar growth – Soltan Think we know quite a bit 5. Radio Mode Know a little 6. Quasar Death - turn-off Ignorant 7. Quiescence Know a little MPIA Heidelberg, July 2011 The Quasar Standard Model MPIA Heidelberg, July 2011 The Quasar Standard Model massive black hole Lynden-Bell 1969 accretion disk Lynden-Bell 1969, Pringle & Rees 1972, Shakura & Sunyaev 1972 relativistic jet Rees 1967 [PhD], Blandford & Rees 1974 MPIA Heidelberg, July 2011 The quasar Spectral Energy Distribution (SED) Elvis et al. 1994 ApJS, 95., 1 ( 1001 citations on 10 Dec 2010 ) Temperature: accretion disk Radio 1 dex IR Opt/UV EUV X-ray Luminosity: Massive Black Hole Elvis et al. 1994 mean SED works in 90%aof Quasars ox (Hao et al. 2011, Harvard PhD 2011) Quasar Growth physics is invariant with z, L, L/LEdd Relativisitic Jet: synchrotron 19 MPIA Heidelberg, July 2011 6 The quasar Standard Model massive black hole Lynden-Bell 1969 accretion disk Lynden-Bell 1969, Pringle & Rees 1972, Shakura & Sunyaev 1972 relativistic jet No prediction of: Atomic Features Maximally Hot dust X-rays Evolution Rees 1967 [PhD], Blandford & Rees 1974 MPIA Heidelberg, July 2011 Age 4: Quasar Growth MPIA Heidelberg, July 2011 Luminosity Function Evolution Traditional approach SDSS Richards et al. (2006) MPIA Heidelberg, July 2011 Quasar Black Hole Masses v2r= r=const GM Keplerian R=L1/2 1 Lag (days) R (cm) 1 2 Black Hole Mass From a single spectrum v2r Vestergaard, 2002 ApJ 571,733 R( rg ) 2 FWHM Peterson & Wandel 1999 Peterson et al. 1993, PASP, 105, 247; 2006MmSAI..77..581P MPIA Heidelberg, July 2011 Black Hole Mass Function vs. Redshift z=2.8 Downsizing Age=2.3Gyr z=1.25 Age=4.9Gyr High Mass Black Holes Turn off Vestergaard et al. (2008) MPIA Heidelberg, July 2011 The Quasar Mass-Luminosity Plane Luminosity Charles Steinhardt, Harvard PhD Thesis 2010 SDSS DR5, all z Kollmeier et al. 2006 Mas Steinhardt s & Elvis 2010 MPIA Heidelberg, July 2011 One M-L slice in redshift 0.2 < z < 0.4, H Luminosity SDSS Saturation Detection Limit Mass MPIA Heidelberg, July 2011 Steinhardt & Elvis 2010 MNRAS, 402, 2637 More physics than just Ledd Longer BH growth times Harder ‘Rapid Growth’ problem 0.2 < z < 0.4, H Luminosity One long ‘on-phase’ allowed? Not episodic outbursts? ~0.5dex Detection Limit MPIA Heidelberg, July 2011 Mas s Steinhardt & Elvis 2010 MNRAS, 402, 2637 Supermassive Black Holes Know about Cosmic Time Boundary moves to higher mass at higher redshift Low z Not just accretion disk physics High z MPIA Heidelberg, July 2011 Steinhardt & Elvis 2010 MNRAS, 402, 2637 Whole Population affected L/LEdd distribution vs. Mass Vertical cuts in M-L plane High mass Low mass Left side of each curve is incomplete Normalized to peak MPIA Heidelberg, July 2011 0.2<z<0.4 Narrow L/Ledd Distribution at fixed redshift, Mass • Common form Normalized to peak • Narrow L/LEdd range • Comparable to variability Intrinsic range is small = Characteristic L//lEdd at each (M,z) ~0.3 dex Are Quasars “Standard candles” after all? Incomplete MPIA Heidelberg, July 2011 More Complex Quasar Growth phase Not all quasars can radiate at the Eddington limit SMBH knows about cosmic time Boundaries move with z Quasars may not be episodic Highest mass quasars at each z are sub-Eddington Could have a single long on-phase At each (z,M) there is a characteristic L/LEdd “Standard Candles”? MPIA Heidelberg, July 2011 Age 6: Quasar Death MPIA Heidelberg, July 2011 Quasar Death: High mass SMBH don’t come back Luminosity Quasar Death line Detection Limit 0.2 < z < 0.4, H MPIA Heidelberg, July 2011 Mas s Death line moves to higher mass with redshift Quasar Death line • In each redshift bin, the highest mass quasars “die” by the next Dz=0.2 bin • Co-ordinated demise: Quasars know about cosmic time 1 Gyr MPIA Heidelberg, July 2011 decline rate of number density depends on mass Log M (solar) 9.75-10.0 Low Mass low M 9.50-9.75 9.25-9.50 9.00-9.25 high High M Mass Steinhardt & Elvis, 2011MNRAS.410..201S MPIA Heidelberg, July 2011 A rapid demise t Gyr -t/t(M) = N0eMasses • Coordinated to <0.7Gyr @ N(t) highest • Set up at z>~10? (Age < 0.5 Gyr) • Declines faster than galaxy mergers? 1 Gyr 9.0 log M/Msol 10 Steinhardt & Elvis, 2011MNRAS.410..201S MPIA Heidelberg, July 2011 Brief High z Star Formation In Massive Galaxies FWHM~100Myr Thomas et al., 2010, MNRAS, 404, 1775 MPIA Heidelberg, July 2011 The Quasar ‘Dying Zone’ Luminosity Quasar Death line Detection Limit 0.2 < z < 0.4, H MPIA Heidelberg, July 2011 Mas s Intrinsically red quasars lie in dying zone Monica Young, Boston University PhD Thesis 2010 z = 1-1.2 z = 1.2-1.4 • 5/7 Red Quasars lie in “turn-off” region z = 1.8-2.0 Young, Steinhardt et al. 2011, in prep. MPIA Heidelberg, July 2011 Red Quasar Fraction Dying (red) Quasars common at highest masses 1.5 < z < 1.7 d(g - i) > 0.3 35% L<0.1LEdd 25% Mas s Young, Steinhardt et al. 2010, in prep. MPIA Heidelberg, July 2011 Quasars die first in UV Strong CIV logM 8.0 Weak CIV zz==1.2-1.4 1-1.2 Larger MgII/CIV at high masses 9.5 Weaker/softer ionizing continuum? 9.0 z~2 Steinhardt & Elvis, 2011MNRAS.410..201S MPIA Heidelberg, July 2011 Low accretion rates in the dying zone Monica Young, Boston University PhD Thesis 2010 Model NOT fit (only normalized) Low mdot low disk temperature T α (MBH.mdot) -1/4 Typical quasar How are emission lines powered? (Elvis+94) Toy model Young, Risaliti & Elvis 2008, ApJ, 688, 128 + Young, et al., in prep. MPIA Heidelberg, July 2011 First Clues to Quasar Death Highest mass quasars at each z fail to reach Eddington limit Quasars die off rapidly above a critical mass at each z Death line moves down in mass toward present Starving the accretion disk may fit ‘dying quasars’ MPIA Heidelberg, July 2011 Age 2: Early Rapid Growth MPIA Heidelberg, July 2011 Evolutionary Tracks for Individual Quasars Initial Mass Steinhardt, Elvis & Amarie, 2011 MNRAS in press, astro-ph/1103.4608 MPIA Heidelberg, July 2011 Tightly Constrained tracks D 20% M0 0.5 dex t0 Mass Luminosity D 20% k a Time Mass k = L/mdot = e/lifetime Steinhardt, Elvis & Amarie, 2011 MNRAS in press, astro-ph/1103.4608 MPIA Heidelberg, July 2011 A Single Track for all SMBH? k = L/mdot = e/lifetime •k small: non-luminous growth dominates, but anti-Soltan •k large: slow growth, smaller turn-off masses Steinhardt, Elvis & Amarie, 2011 MNRAS in press, astro-ph/1103.4608 MPIA Heidelberg, July 2011 A single track for ALL Quasars ? Invert MgII masses only to give z>0.8, t0 < SMBH 6 Gyr Initial Mass Function? No exponential solutions •: >0.2dex from boundary • Interpolation issues Steinhardt, Elvis & Amarie, 2010 MNRAS in press, astro-ph/1103.4608 MPIA Heidelberg, July 2011 First Clues to Quasar Initial growth Quasars must stay within M,L locus Simple evolutionary tracks can achieve this A single evolutionary track for all quasars is allowed Invert to get SMBH IMF? MPIA Heidelberg, July 2011 The 7 Ages of Supermassive Black Holes: What have we learned? 1. Birth Ignorant 2. Rapid growth Initial Mass Function? No data 3. Merger growth Know a little 4. Quasar growth L ≠ Ledd ; knows z; standard candle? Think we know quite a bit 5. Radio Mode Know a little 6. Quasar Death Rapid, Ignorantcoordinated; starvation? 7. Quiescence Know a little Quasar Mass-Luminosity Plane is a valuable tool MPIA Heidelberg, July 2011 All the world's a stage, And all the men and women merely players; They have their exits and their entrances; And one man in his time plays many parts, His acts being seven ages. At first the infant, Mewling and puking in the nurse's arms; And then the whining school-boy, with his satchel And shining morning face, creeping like snail Unwillingly to school. And then the lover, Sighing like furnace, with a woeful ballad Made to his mistress' eyebrow. Then a soldier, Full of strange oaths, and bearded like the pard, Jealous in honour, sudden and quick in quarrel, Seeking the bubble reputation Even in the cannon's mouth. And then the justice, In fair round belly with good capon lin'd, With eyes severe and beard of formal cut, Full of wise saws and modern instances; And so he plays his part. The sixth age shifts Into the lean and slipper'd pantaloon, With spectacles on nose and pouch on side; His youthful hose, well sav'd, a world too wide For his shrunk shank; and his big manly voice, Turning again toward childish treble, pipes And whistles in his sound. Last scene of all, That ends this strange eventful history, Is second childishness and mere oblivion; Sans teeth, sans eyes, sans taste, sans everything. The Seven ages of man MPIA Heidelberg, July 2011 Jaques; As You Like It, Act II, Scene VII, lines 139-166’ William Shakespeare S. Harris Postscript: Accretion Disk Winds MPIA Heidelberg, July 2011 Atomic Features in Quasar Spectra None are predicted by the Quasar Standard Model High ionization BELs e.g. CIV, OVI Low ionization BELs e.g. MgII, H. MPIA Heidelberg, July 2011 Radiation Driving Determines Quasar Structure Elvis 2000ApJ...545...63E; Risaliti & Elvis, 2010, A&A 516, A 89 High Ionization Absorber (failed) electronscattering wind Warm Absorber/ High ionization BLR Line-Driven wind Cold Eclipsers/ Low ionization BLR Failed wind MPIA Heidelberg, July 2011 Slow Cold Eclipsers Dust-Driven Wind NLR Bicones Broad Absorption Lines Accretion Disk Winds: the 4th Element Explains ALL Emission & Absorption Lines Explains: Broad, Narrow Absorption Lines, High Ionization Emission Lines, hot dust Still no prediction of: massive black hole X-rays Lynden-Bell 1969 accretion disk Evolution: The 7 Ages of BH Lynden-Bell 1969, Pringle & Rees 1972, Shakura & Sunyaev 1972 relativistic jet Rees 1967 [PhD], Blandford & Rees 1974 disk winds Murray et al., 1995 Elvis 2000 Nenkova et al., 2008 MPIA Heidelberg, July 2011 PS2: Merger Growth MPIA Heidelberg, July 2011 Merger Growth: Hot-Dust Poor QUASARS Heng Hao, Harvard PhD Thesis 2011 Hao et al. 2010 ApJ Low Covering Factor (0.06-0.3) Missing inner ‘torus’ z<1.5 1.5<z<3 merger-related cause: 4.9%±0.8% 15.9%±3% E94 Timing suggests • Disrupted ‘torus’? 0.3-0.6 • Outburst destroyed inner dust? dex • Merger ejected SMBH+disk+BLR, not ‘torus’? (Komossa & Merritt 2006; Guedes et al., 2010) MPIA Heidelberg, July 2011 Merger Growth in action: a Recoiling Black Hole Civano et al. 2010 ApJ Chandra COSMOS source CID-42 [OIII] N z=0.359 E H H Off-nuclear source Is the “AGN” Dv=1180km/s 2.5kpc by Eli Bressert 15” MPIA Heidelberg, July 2011